“…The datasets that we use for this calculation are mock future supernova (SN) datasets as might be expected from the WFIRST telescope [8,30] and future baryon acoustic oscillation (BAO) datasets as might be expected from DESI [6,7] Type Ia SN are one of the observational pillars that built the ΛCDM model and directly measure the acceleration of the Universe. Existing SN datasets have all shown broad consistency with the ΛCDM model despite concerted searches for new physics or systematics [2,3,9,14,15,18,19,23,25,26,29,31]. These successes of SN exist because they are standardizable candles; the measurement and fitting of the light-curve of the SN allows us to infer the luminosity of the SN (up to a global calibration) [2,3,9,18,23,25,26,29,31], and thus measuring the flux is equivalent to measuring a luminosity distance, or equivalently a distance moduli:…”